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Fig. 10


Distributions of initial and final solar orbits for all our simulations using the full dynamical model. Pericentre (q) and apocentre (Q) distances of the rosette orbits are plotted on the axes of each diagram. Left panels: the high-mass cluster. Right panels: the intermediate-mass cluster. Top panels: initial orbits. For the HM cluster, these orbits start from the half-mass radius (r = 4.87 pc) with some random radial velocity, so we always have q< 4.87 pc <Q. The red crosses denote orbits, where the Sun was ejected from the cluster during the simulation, while the rest are denoted by black diamonds. Bottom panels: final orbits. Only orbits where the Sun survived as a cluster member are shown.

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